Cooling+ Heating Flows in Galaxy Clusters: Turbulent Heating, Spectral
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Dynamics of Hot Gas in Galaxies, Groups, & Clusters
DynamicsDynamics ofof hothot gasgas inin Galaxies,Galaxies, Groups,Groups, && ClustersClusters Bill Mathews Colleagues: Fabrizio Brighenti (Bologna) David Buote (UC Irvine) X-ray images of groups and clusters of galaxies Conventional cooling flows Evidence that cooling flows are not cooling as expected Proposed explanations why cooling flows aren’t cooling Heating cluster gas with AGN energy by dissipation of weak shock waves by PdV work as X-ray cavities form Cosmic ray buoyancy and outward gas circulation TypicalTypical HotHot GasGas ParametersParameters E galaxies rich galaxy & groups clusters Temperature 107 108 K X-ray luminosity 1039-44 1043-46 erg/s Fe abundance 0.4-1.0 0.4 solar 12-13 14-15 Total mass 10 10 Msun Baryon fraction < 0.16 ~0.16 XMMXMM ImageImage ofof PerseusPerseus ClusterCluster X-ray contours kpc 220 200ks Chandra image is here (Churazov et al. 2003) Central active cD galaxy 14 virial mass: Mvir = 8.5x10 Msun NGC 1275 DeepDeep 200ks200ks ChandraChandra ImageImage ofof PerseusPerseus ClusterCluster X-ray cavities -- bubbles (Fabian et al. 2003) Distance 73 Mpc 45 Lx 10 erg/s kpc 22 22 Absorption from foreground gas in merging galaxy Deprojected Deprojected XMM Observationsof XMM Observationsof this region affected by AGN core emission (Churazov Perseus Perseus et al.2003) averaged azimuthally Cluster Cluster 200ks Chandra Observations in Perseus strange radial abundance gradients less accurate only Ne peaks less accurate in the core 0 r (kpc) 120 (Sanders et al. 2004) Many elements have strange off-center peaks Abundance patterns are similar in Virgo (M87) ChandraChandra andand RadioRadio ImagesImages ofof PerseusPerseus radio contours (Fabian et al. -
Arxiv:1904.08942V1 [Astro-Ph.GA] 18 Apr 2019
Draft version April 22, 2019 Preprint typeset using LATEX style emulateapj v. 01/23/15 ANATOMY OF A COOLING FLOW: THE FEEDBACK RESPONSE TO PURE COOLING IN THE CORE OF THE PHOENIX CLUSTER M. McDonald1, B. R. McNamara2, G. M. Voit3, M. Bayliss1, B. A. Benson4,5,6, M. Brodwin7, R. E. A. Canning8,9, M. K. Florian10, G. P. Garmire11, M. Gaspari12,y, M. D. Gladders5,6, J. Hlavacek-Larrondo13, E. Kara1,14, C. L. Reichardt15, H. R. Russell16, A. Saro17,18,19, K. Sharon20, T. Somboonpanyakul1, G. R. Tremblay21, R. J. van Weeren22 Draft version April 22, 2019 ABSTRACT We present new, deep observations of the Phoenix cluster from the Chandra X-ray Observatory, the Hubble Space Telescope, and the Karl Jansky Very Large Array. These data provide an order of magnitude improvement in depth and/or angular resolution at X-ray, optical, and radio wavelengths, yielding an unprecedented view of the core of the Phoenix cluster. We find that the one-dimensional temperature and entropy profiles are consistent with expectations for pure-cooling hydrodynamic simulations and analytic descriptions of homogeneous, steady-state cooling flow models. In particular, the entropy profile is well-fit by a single power law at all radii, with no evidence for excess entropy in the core. In the inner ∼10 kpc, the cooling time is shorter by an order of magnitude than any other known cluster, while the ratio of the cooling time to freefall time (tcool=tff ) approaches unity, signaling that the ICM is unable to resist multiphase condensation on kpc scales. -
X-Ray Spectroscopy of Cooling Clusters
SLAC-PUB-11612 January 2006 astro-ph/0512549 X-ray Spectroscopy of Cooling Clusters J. R. Peterson a,1 & A. C. Fabian b,2 aKavli Institute for Particle Astrophysics and Cosmology (KIPAC), Stanford University, PO Box 20450, Stanford, CA 94309, USA bInstitute of Astronomy (IoA), Cambridge University, Madingley Road, Cambridge CB3 0HA, UK Abstract We review the X-ray spectra of the cores of clusters of galaxies. Recent high resolu- tion X-ray spectroscopic observations have demonstrated a severe deficit of emission at the lowest X-ray temperatures as compared to that expected from simple radia- tive cooling models. The same observations have provided compelling evidence that the gas in the cores is cooling below half the maximum temperature. We review these results, discuss physical models of cooling clusters, and describe the X-ray instrumentation and analysis techniques used to make these observations. We dis- cuss several viable mechanisms designed to cancel or distort the expected process of X-ray cluster cooling. Submitted to Physics Reports 1 JRP E-mail: [email protected] 2 ACF E-mail: [email protected] Work supported in part by Department of Energy contract DE-AC02-76SF00515 KIPAC, SLAC, Stanford Univesity, Stanford, CA 94309 Contents 1 Introduction 4 2 Clusters of Galaxies 5 3 Physics of the Intracluster Medium 7 3.1 X-ray Emission from Collisional Plasmas 7 3.2 Magneto-hydrodynamics 15 3.3 Cooling flows 18 4 X-ray Instrumentation and Observational Techniques 24 4.1 X-ray Telescopes and their Relevance to Clusters 24 4.2 Analysis -
Feedback from Active Galactic Nuclei in Galaxy Groups
universe Review Feedback from Active Galactic Nuclei in Galaxy Groups Dominique Eckert 1,*,† , Massimo Gaspari 2,3,† , Fabio Gastaldello 4,† , Amandine M. C. Le Brun 5,† and Ewan O’Sullivan 6,† 1 Department of Astronomy, University of Geneva, Ch. d’Ecogia 16, CH-1290 Versoix, Switzerland 2 INAF—Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero Gobetti 93/3, I-40129 Bologna, Italy; [email protected] 3 Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA 4 IASF—Milano, INAF, Via A. Corti 12, I-20133 Milano, Italy; [email protected] 5 LUTh, UMR 8102 CNRS, Observatoire de Paris, PSL Research University, Université Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France; [email protected] 6 Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA; [email protected] * Correspondence: [email protected] † All authors contributed equally to this work. Abstract: The co-evolution between supermassive black holes and their environment is most directly traced by the hot atmospheres of dark matter halos. The cooling of the hot atmosphere supplies the central regions with fresh gas, igniting active galactic nuclei (AGN) with long duty cycles. Outflows from the central engine tightly couple with the surrounding gaseous medium and provide the dominant heating source preventing runaway cooling by carving cavities and driving shocks across the medium. The AGN feedback loop is a key feature of all modern galaxy evolution models. Here, we review our knowledge of the AGN feedback process in the specific context of galaxy groups. -
Abstract Handbook
Scientific Organizing Committee: SOC Chair: Jan Vrtilek (SAO) Steve Allen (KIPAC) Liz Blanton (B.U.) Marcus Brueggen (Jacobs University) Eugene Churazov (MPA) Megan Donahue (Michigan State) Luigina Feretti (Bologna) Ralph Kraft (SAO) Kasuhisa Mitsuda (ISAS/JAXA) Paul Nulsen (SAO) Ewan O’Sullivan (Univ. of Birmingham, UK) Local Organizing Committee: Chair: Paul Green Michelle Henson Lauren Deknis Bortolami Ryan Foltz Evan Tingle Lisa Paton This Chandra science workshop is sponsored by the Chandra Directors Office (CDO) at the Chandra X-ray Center (CXC), part of the Smithsonian Astrophysical Observatory in Cambridge, MA. Tuesday July 12 8:45 - 9:00 Opening Remarks I. Cluster Structure Since 2000, What Has Chandra Seen and How Has it Changed Our Views? 9:00 - 9:30 Craig Sarazin Chandra’s Clear View of the Structure of Clusters 9:30 - 9:45 William Forman A Shock Model for the the Outburst from the Supermassive Black Hole in M87 9:45 - 10:00 Elizabeth Blanton Sloshing, Shocks and Bubbles in the Cool Core Cluster Abell 2052 10:00 - 10:30 Poster Microtalks 10:30 - 11:00 Break and Poster Viewing II. Cluster and Group Physics - Gas Dynamics, Transport Properties, Outstanding Questions 11:00 - 11:30 Eugene Churazov X-ray Surface Brightness Fluctuations and ICM Physics 11:30 - 11:45 Jelle de Plaa Turbulence Measurements in Two Giant Elliptical Galaxies 11:45 - 12:00 Jeremy Lim Velocity Field of the Optical Nebula at the Center of the Perseus Cluster 12:00 - 12:15 Takayuki Tamura Discovery of Gas Bulk Motion in the Galaxy Cluster Abell 2256 with Suzaku 12:15 - 12:30 Helen Russell Revealing the ICM transport properties with a deep Chandra observation of A2146 12:30 - 2:00 Lunch and Poster Viewing III. -
Regulation of Star Formation Amidst Heating and Cooling in Galaxies and Galaxy Clusters
Rochester Institute of Technology RIT Scholar Works Theses 8-2016 Regulation of Star Formation Amidst Heating and Cooling in Galaxies and Galaxy Clusters Sravani Vaddi [email protected] Follow this and additional works at: https://scholarworks.rit.edu/theses Recommended Citation Vaddi, Sravani, "Regulation of Star Formation Amidst Heating and Cooling in Galaxies and Galaxy Clusters" (2016). Thesis. Rochester Institute of Technology. Accessed from This Dissertation is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Theses by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Regulation of Star Formation amidst Heating and Cooling in Galaxies and Galaxy Clusters by Sravani Vaddi A dissertation submitted in partial fulfillment of the requirements for the degree of Ph.D. in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Rochester Institute of Technology August, 2016 Approved by Dr. Andrew Robinson Date Director, Astrophysical Sciences and Technology Astrophysical Sciences and Technology College of Science Rochester Institute of Technology Rochester, New York, USA Certificate of Approval Ph.D. Degree Dissertation The Ph.D. Degree Dissertation of SRAVANI VADDI has been examined and approved by the dissertation committee as satisfactory for the dissertation requirement for the Ph.D. degree in Astrophysical Sciences and Technology. Dr. Chris O’Dea, Dissertation Advisor Date Dr. Stefi Baum, Dissertation Advisor Date Dr. Anthony Vodacek, Committee Chair Date Dr. Alice Quillen Date Dr. Andrew Robinson Date To all my teachers who believed in me and supported me all through my life. -
Harvard-Smithsonian 0 Center for Astrophyslcs
- Harvard-Smithsonian 0 Center for Astrophyslcs Preprint Series No. 4621 (Received November 19, 1997) THE EVOLUTION OF GAS AND STARS IN THE MERGER GALAXY NGC 1316 (FORNAX A) G. Mackie and G. Fabbiano Harvard-Smithsonian Center for Astrophysics To appear in Astronomical Journal February 1998 HARVARD COLLEGE OBSERVATORY SMITHSONIANASTROPHYSICALOBSERVATORY 60 Garden Street, Cambridge, Massachusetts 02138 An X-ray Catalog and Atlas of Galaxies by G. Fabbiano, D-W. Kim, and G. Trinchieri, Ap.J.Suppl. 1992, 80, 531-644. The X-ray spectra of Galaxies: I. Spectral Fits of Individual Galaxies and X-ray Colors by D-W. Kim, G. Fabbiano, and G. Trinchieri, Ap.J.Suppl. 1992, 80, 531. The X-ray Spectra of Galaxies: II. Average Spectral Properties and Emission Mechanisms by D-W. Kim, G. Fabbiano and G. Trinchieri, Ap.J. 1992, 393, 134. Prepints are attached. *A Multiparametric Analysis of the Einstein Sample of Early-type Galaxies. II: Galaxy Formation History and Properties of the ISM by P. Eskridge, G. Fabbiano, and D-W. Kim, Ap.J. 1995, 442, 2. *A Multiparametric Analysis of the Einstein Sample of Early-type Galaxies. III: Compar- isons with the t_ Parameters, Ap.J. 1995, 448, 7-. *ROSAT PSPC Observations of NGC 507/499: Central Cooling and Mass Determination, by D-W. Kim, and G. Fabbiano, Ap.J., 1995, 441,182. *ROSAT PSPC Observations of Two Dynamically Young Elliptical Galaxies: NGC 4125 and NGC 3610 by G. Fabbiano and F. Schweizer, Ap.J. 1995, 447, 572. ASCA Spectra of the X-ray Faint SO Galaxy NGC 4382 by D-W. -
Mechanical Feedback from Active Galactic Nuclei in Galaxies, Groups and Clusters
PAPER Related content - The Starburst in the Abell 1835 Cluster Mechanical feedback from active galactic nuclei in Central Galaxy: A Case Study of Galaxy Formation Regulated by an Outburst from a Supermassive Black Hole galaxies, groups and clusters B. R. McNamara, D. A. Rafferty, L. Bîrzan et al. To cite this article: B R McNamara and P E J Nulsen 2012 New J. Phys. 14 055023 - An Energetic AGN Outburst Powered by a Rapidly Spinning Supermassive Black Hole or an Accreting Ultramassive Black Hole B. R. McNamara, F. Kazemzadeh, D. A. View the article online for updates and enhancements. Rafferty et al. - Average Heating Rate of Hot Atmospheres in Distant Clusters by Radio Active Galactic Nucleus: Evidence for Continuous Active Galactic Nucleus Heating C.-J. Ma, B. R. McNamara, P. E. J. Nulsen et al. Recent citations - AGN jet feedback on a moving mesh: gentle cluster heating by weak shocks and lobe disruption Martin A Bourne and Debora Sijacki - Constraining the AGN duty cycle in the cool-core cluster MS 0735.6+7421 with LOFAR data Nadia Biava et al - The Metal Content of the Hot Atmospheres of Galaxy Groups Fabio Gastaldello et al This content was downloaded from IP address 170.106.202.126 on 25/09/2021 at 10:19 New Journal of Physics The open–access journal for physics Mechanical feedback from active galactic nuclei in galaxies, groups and clusters B R McNamara1,2,3,4 and P E J Nulsen3,4 1 Department of Physics and Astronomy, University of Waterloo, Waterloo, ON, Canada 2 Perimeter Institute for Theoretical Physics, Waterloo, ON, Canada 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA E-mail: [email protected] and [email protected] New Journal of Physics 14 (2012) 055023 (40pp) Received 30 November 2011 Published 23 May 2012 Online at http://www.njp.org/ doi:10.1088/1367-2630/14/5/055023 Abstract. -
Active Galactic Nucleus Feedback in Clusters of Galaxies
Active galactic nucleus feedback in clusters of galaxies Elizabeth L. Blantona,1, T. E. Clarkeb, Craig L. Sarazinc, Scott W. Randalld, and Brian R. McNamarad,e aInstitute for Astrophysical Research and Astronomy Department, Boston University, 725 Commonwealth Avenue, Boston, MA 02215; bNaval Research Laboratory, 455 Overlook Avenue SW, Washington, DC 20375; cDepartment of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325; dHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; eDepartment of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 2G1, Canada; and Perimeter Institute for Theoretical Physics, 31 Caroline Street, North Waterloo, Ontario N2L 2Y5, Canada Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved February 22, 2010 (received for review December 3, 2009) Observations made during the last ten years with the Chandra there is little cooling. This is seen in the temperature profiles as X-ray Observatory have shed much light on the cooling gas in well as high resolution spectroscopy. An important early result the centers of clusters of galaxies and the role of active galactic from XMM-Newton high resolution spectra from cooling flows nucleus (AGN) heating. Cooling of the hot intracluster medium was that the emission lines from cool gas were not present at in cluster centers can feed the supermassive black holes found the expected levels, and the spectra were well-fitted by a cooling in the nuclei of the dominant cluster galaxies leading to AGN out- flow model with a low temperature cutoff (7, 8). This cutoff is bursts which can reheat the gas, suppressing cooling and large typically one-half to one-third of the average cluster temperature, amounts of star formation. -
Active Galactic Nucleus Feedback in Clusters of Galaxies
Active galactic nucleus feedback in SPECIAL FEATURE clusters of galaxies Elizabeth L. Blantona,1, T. E. Clarkeb, Craig L. Sarazinc, Scott W. Randalld, and Brian R. McNamarad,e aInstitute for Astrophysical Research and Astronomy Department, Boston University, 725 Commonwealth Avenue, Boston, MA 02215; bNaval Research Laboratory, 455 Overlook Avenue SW, Washington, DC 20375; cDepartment of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325; dHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; eDepartment of Physics and Astronomy, University of Waterloo, Waterloo, ON N2L 2G1, Canada; and Perimeter Institute for Theoretical Physics, 31 Caroline Street, North Waterloo, Ontario N2L 2Y5, Canada Edited by Neta A. Bahcall, Princeton University, Princeton, NJ, and approved February 22, 2010 (received for review December 3, 2009) Observations made during the last ten years with the Chandra there is little cooling. This is seen in the temperature profiles as X-ray Observatory have shed much light on the cooling gas in well as high resolution spectroscopy. An important early result the centers of clusters of galaxies and the role of active galactic from XMM-Newton high resolution spectra from cooling flows nucleus (AGN) heating. Cooling of the hot intracluster medium was that the emission lines from cool gas were not present at in cluster centers can feed the supermassive black holes found the expected levels, and the spectra were well-fitted by a cooling in the nuclei of the dominant cluster galaxies leading to AGN out- flow model with a low temperature cutoff (7, 8). This cutoff is bursts which can reheat the gas, suppressing cooling and large typically one-half to one-third of the average cluster temperature, amounts of star formation.